The Magellan PFS planet search program: radial velocity and stellar abundance analyses of the 360 au, metal-poor binary "Twins" HD 133131A & B

Abstract

We present a new precision radial velocity (RV) data set that reveals multiple planets orbiting the stars in the similar to 360 au, G2+G2 "twin" binary HD 133131AB. Our six years of high-resolution echelle observations from MIKE and five years from the Planet Finder Spectrograph (PFS) on the Magellan telescopes indicate the presence of two eccentric planets around HD 133131A with minimum masses of 1.43 +/- 0.03 and 0.63 +/- 0.15 M-J at 1.44 +/- 0.005 and 4.79 +/- 0.92 au, respectively. Additional PFS observations of HD 133131B spanning five years indicate the presence of one eccentric planet of minimum mass 2.50 +/- 0.05 M-J at 6.40 +/- 0.59 au, making it one of the longest-period planets detected with RV to date. These planets are the first to be reported primarily based on data taken with the PFS on Magellan, demonstrating the instrument's precision and the advantage of long-baseline RV observations. We perform a differential analysis between the Sun and each star, and between the stars themselves, to derive stellar parameters and measure a suite of 21 abundances across a wide range of condensation temperatures. The host stars are old (likely similar to 9.5 Gyr) and metal-poor ([Fe/ H] similar to -0.30), and we detect a similar to 0.03 dex depletion in refractory elements in HD 133131A versus B (with standard errors similar to 0.017). This detection and analysis adds to a small but growing sample of binary "twin" exoplanet host stars with precise abundances measured, and represents the most metal-poor and likely oldest in that sample. Overall, the planets around HD 133131A and B fall in an unexpected regime in planet mass-host star metallicity space and will serve as an important benchmark for the study of long-period giant planets.